Different simulations show that the born-again star can stay inflated, i.e., \(R \gg 1 R_\odot \)  (e.g., [1]}) for hundreds of years (e.g.,
[2]}, [3]}, [4]}).
However, more massive stars at the time of LTP/VLTP evolve faster (e.g., [5]}, [6]}). On top of these, the time of evolution depends on the uncertain efficiency of convective mixing of elements (e.g., [7]}, [2]}), and the evolution time seems to be short (e.g., [7]}, [10]}), down to several years (e.g., [11]}). Overall, I scale the WD-inflated phase after a LTP/VLTP with a time scale of \(\tau _{BA} \approx 100 {~\rm yr}\) , but it might be shorter even. This implies that only \(1 \%\)  of the SNe Ia that explode within \(10^4 - 10^5 {~\rm yr}\)  from the termination of the AGB will take place inside a born-again envelope. With equation (REF ) I conclude that the fraction of SN Ia inside an inflated born-again envelope is extremely low
\(N_{\rm BA,SN} < {\rm few} \times 10^{-4} N_{\rm Ia}.\) 
